The evolution of the U Orionis OH masers has been followed for several years. The 1612 MHz maser emission has continued to decline in the damped oscillator mode previously reported. The main lines masers, in contrast, have become stronger in recent years and are varying with the stellar cycle. Their emission curves show an unusual, sharply peaked form, however. Observations obtained by other investigators are plotted with our own to form a comprehensive display of the behavior of these masers. An interpretation of the evolution is given, and the implications of this source for OH masers and circumstellar shells in general are discussed.